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pclm_scripts.tar
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pclm_Fig1a_mieattn.py 0000644 0501442 0003262 00000005257 14326611354 014405 0 ustar u0095165 bromley import numpy as np
import scatter as sc
import pylab as pl
from scipy.optimize import root_scalar
from scipy.interpolate import interp1d
import time
import os
from nbody import *
import myfig
import attnmie
from myparms import *
from constants import *
#import miepython
#def do_attn(Mdust,dustradius,rho,nindex):
# global Lsolar,Msolar,Rsolar,Mearth,des,G,c
# qext, qsca, g = do_mie(dustradius,nindex)
# qpr = qext-g*qsca
# beta = 3*Lsolar*qpr/(16*np.pi*G*c*rho*dustradius*Msolar)
# d1 = get_d1(Msolar,Mearth,des,np.zeros(dustradius.shape),G)
# rshadow = Rsolar*d1/(des-d1)
# fshadow = Rearth**2/rshadow**2
# msk = d1<0
# fshadow[msk] = 0.0
# attn = np.zeros(dustradius.shape)
# attn = fshadow * qext * dustradius**2 * des**2/ Rsolar**2/ d1**2 * Mdust/(4/3*np.pi*rho*dustradius**3)
# return attn, beta, d1
#ncoal = 1.85-0.23j; rhocoal = 1.4 # coal McCartney et al 1965 Fuel 44, 349
#nsalt = 1.5 - 1e-6j; rhosalt = 2.0
#nsand = 1.45 - 1e-7j; rhosand = 2.7
#nglass = 1.51 - 1e-8j; rhoglass = 2.51
#ngold = 0.27 - 2.92j; rhogold = 19.3
#nal = 1.37 - 7.6j; rhoal = 2.7
#nolivine = 1.67 - 1e-3j; rhoolivine = 2.7 # D. Fabian, Th. Henning, C. Jäger, H. Mutschke, J. Dorschner, O. Werhan, Astron. Astrophys. 378, 228 (2001).
#print('# n:',nindex,G,c)
nlis = [nsalt,ncoal,nolivine,nal,ngold]
slis = ['sea salt','coal dust','lunar dust','aluminum spheres','gold spheres']
rholis = [rhosalt,rhocoal,rhoolivine,rhoal,rhogold]
clis = ['#8888ff','#000000','#226600','#aaaaaa','#c7a033']
nr = 100
dustradius = np.logspace(np.log10(0.0007*micron),np.log10(1200*micron),nr)
#Mdust = 5e11
d1 = attnmie.get_d1(Msolar,Mearth,AU,0,GNewt)
zo=1
for nindex, stuff, rho, color in zip(nlis,slis,rholis,clis):
mp = 4*np.pi/3*rho*dustradius**3
qext,_,_ = attnmie.do_mie(dustradius,nindex)
attn = attnmie.attnscatter(dustradius,qext,0.0,d1,asemi=AU,Ndust=Mdust/mp)
pl.loglog(dustradius/micron,attn,'-',lw=2, label=stuff, c=color,zorder=zo)
rball = (Mdust/(4*np.pi/3*rho))**(1/3)
print('rball (m):',rball/1e2,rho)
zo+=1
pl.xlim((dustradius[0]/micron,dustradius[-1]/micron))
pl.ylim(7e-6,3e-1)
xx, yy = [dustradius[0]/micron,dustradius[-1]/micron], [attnlevel]*2
xx, yy = [3e-3,2], [attnlevel]*2
pl.loglog(xx,yy,'--',c='#777777',zorder=0)
pl.xlabel(r'particle radius ($\mu$m)')
pl.ylabel(r'attenuation')
pl.figtext(0.18,0.8,r'cloud mass: '+Mduststr)
pl.legend(loc = 'upper right')
ofil = 'mieattn.pdf'
pl.savefig(ofil)
ofil = 'mieattn.pdf'
pl.savefig(ofil)
myscript = __file__
fignm = myscript.split('_')[1]
print(fignm)
pl.savefig(fignm+".pdf")
import os
os.system('convert '+ofil+' ~/www/tmp.tiff')
pclm_Fig1b_mieattndesigner.py 0000644 0501442 0003262 00000010676 14326610340 016122 0 ustar u0095165 bromley import numpy as np
import pylab as pl
from scipy.optimize import root_scalar
from scipy.interpolate import interp1d
import time
import os
import myfig
import attnmie
from constants import *
from myparms import *
nindex = nglass; rho = rhoglass
G = GNewt
c = clight
des = AU
nr = 100
# dustradius is volumne equiv radius
dustradius = np.logspace(np.log10(0.007*micron),np.log10(800*micron),nr)
dustVol = 4*np.pi/3*dustradius**3
mdust = dustVol*rho
# dustVol = np.pi*(dustD/2)**3*asp
aspect = [30,300]; clis = ['brown','goldenrod']
aspect = [100]; clis = ['goldenrod']
for asp,col in zip(aspect,clis):
dustD = (dustVol/np.pi/asp)**(1/3)
dustL = asp*dustD
Aproj = dustL*dustD*0.785
radAreaEquiv = np.sqrt(Aproj/np.pi)
radVolEquiv = dustradius
# qext, qsca, g = attnmie.do_mie(radAreaEquiv,nindex)
qext, qsca, g = attnmie.do_mie(radVolEquiv,nindex) # could use area-equiv...
qpr = qext-g*qsca
beta = Lsolar*qpr*radAreaEquiv**2/(4*G*c*(dustVol*rho)*Msolar)
d1 = attnmie.get_d1(Msolar,Mearth,des,0*beta,G)
rshadow = Rsolar*d1/(des-d1)
fshadow = Rearth**2/rshadow**2
msk = d1<0
fshadow[msk] = 0.0
attn = fshadow * qext * (radAreaEquiv/Rearth)**2 * Mdust/(dustVol*rho)
pl.loglog(dustradius/micron,attn,'-',lw=2, c=col,label='rod (%g:1)'%(asp))
# dustVol = np.pi*(dustD/2)**3*asp
aspect = [30,300]; clis = ['darkviolet','violet']
aspect = [100]; clis = ['darkviolet']
for asp,col in zip(aspect,clis):
cylthick = 0.2 # frac of radius
ff = 1-(1-cylthick)**2 # filling frac, hollow cylinder
print('ff',ff)
dustD = (dustVol/np.pi/asp/ff)**(1/3)
dustL = asp*dustD
ef = np.real(nindex)**2
fff = lambda x: (1-ff)*(1-x)/(1+2*x)+ff*(ef-x)/(ef+2*x)
neff = np.sqrt(root_scalar(fff,x0=1,x1=ef,rtol=1e-8).root)
Aproj = dustL*dustD*0.785
radAreaEquiv = np.sqrt(Aproj/np.pi)
radVolEquiv = dustradius
# qext, qsca, g = attnmie.do_mie(radAreaEquiv,nindex)
qext, qsca, g = attnmie.do_mie(radVolEquiv,neff) # could use area-equiv...
qpr = qext-g*qsca
beta = Lsolar*qpr*radAreaEquiv**2/(4*G*c*(dustVol*rho)*Msolar)
d1 = attnmie.get_d1(Msolar,Mearth,des,0*beta,G)
rshadow = Rsolar*d1/(des-d1)
fshadow = Rearth**2/rshadow**2
msk = d1<0
fshadow[msk] = 0.0
attn = fshadow * qext * (radAreaEquiv/Rearth)**2 * Mdust/(dustVol*rho)
pl.loglog(dustradius/micron,attn,'-',lw=2, c=col,label='tube (%g:1:%g)'%(asp,cylthick/2))
flufffill = [0.5,0.1]
clis = ['#4477aa','#99aaff']
for ff,col in zip(flufffill,clis):
ef = np.real(nindex)**2
fff = lambda x: (1-ff)*(1-x)/(1+2*x)+ff*(ef-x)/(ef+2*x)
neff = np.sqrt(root_scalar(fff,x0=1,x1=ef,rtol=1e-8).root)
# for this radius, the eff vall radius, find the physics radius....
# Vfluff = f*Veff so
rfluff = dustradius/ff**(1/3)
qext, qsca, g = attnmie.do_mie(rfluff,neff) # could use area-equiv...
qpr = qext-g*qsca
mdust = 4*np.pi/3*dustradius**3*rho
beta = Lsolar*qpr*rfluff**2/(4*G*c*mdust*Msolar)
d1 = attnmie.get_d1(Msolar,Mearth,des,0*beta,G)
rshadow = Rsolar*d1/(des-d1)
fshadow = Rearth**2/rshadow**2
msk = d1<0
fshadow[msk] = 0.0
attnf = fshadow * qext * (rfluff/Rearth)**2 * Mdust/mdust
pl.loglog(dustradius/micron,attnf,'-',lw=2, c=col,label='fluff ball (%g)'%(ff),zorder=99)
qext, qsca, g = attnmie.do_mie(dustradius,nindex) # could use area-equiv...
qpr = qext-g*qsca
mdust = 4*np.pi/3*dustradius**3*rho
beta = Lsolar*qpr*dustradius**2/(4*G*c*mdust*Msolar)
d1 = attnmie.get_d1(Msolar,Mearth,des,0*beta,G)
rshadow = Rsolar*d1/(des-d1)
fshadow = Rearth**2/rshadow**2
msk = d1<0
fshadow[msk] = 0.0
attns = fshadow * qext * (dustradius/Rearth)**2 * Mdust/mdust
pl.loglog(dustradius/micron,attns,'-',lw=2, c='k',label='solid sphere')
rball = (Mdust/(4*np.pi/3*rho))**(1/3)
print('rball (m):',rball/1e2,rho)
pl.figtext(0.18,0.8,r'cloud mass: '+Mduststr)
pl.xlim((dustradius[0]/micron,dustradius[-1]/micron))
pl.ylim(7e-6,3e-1)
xx, yy = [dustradius[0]/micron,dustradius[-1]/micron], [attnlevel]*2
xx, yy = [3e-2,4], [attnlevel]*2
pl.loglog(xx,yy,'--',c='#777777',zorder=0)
pl.xlabel(r'particle radius ($\mu$m)')
pl.ylabel(r'attenuation')
pl.legend(loc='upper right')
ofil = 'mieattndesigner.pdf'
pl.savefig(ofil)
myscript = __file__
fignm = myscript.split('_')[1]
print(fignm)
pl.savefig(fignm+".pdf")
import os
os.system('convert '+ofil+' ~/www/tmp.tiff')
pclm_Fig2_halojpl.py 0000644 0501442 0003262 00000050642 14326612042 014226 0 ustar u0095165 bromley #
import numpy as np
import pandas as pd
from scipy.optimize import minimize
from scipy.interpolate import interp1d
import time
import pylab as pl
import os
import glob
from nbody import *
import scatter as sc
import myfig
def setorb(b,drdv,tracerindex=3): # reconsider returning, not this crap
xs,ys,zs = b[0].x,b[0].y,b[0].z
vxs,vys,vzs = b[0].vx,b[0].vy,b[0].vz
# work in sun frame
xem = np.sum((b[1:3].x-xs)*b[1:3].m)/np.sum(b[1:3].m)
yem = np.sum((b[1:3].y-ys)*b[1:3].m)/np.sum(b[1:3].m)
zem = np.sum((b[1:3].z-zs)*b[1:3].m)/np.sum(b[1:3].m)
rem = np.sqrt(xem**2+yem**2+zem**2)
vxem = np.sum((b[1:3].vx-vxs)*b[1:3].m)/np.sum(b[1:3].m)
vyem = np.sum((b[1:3].vy-vys)*b[1:3].m)/np.sum(b[1:3].m)
vzem = np.sum((b[1:3].vz-vzs)*b[1:3].m)/np.sum(b[1:3].m)
#dr0 = -rem*(b[1].m/3/b[0].m)**(1/3)
dr0fid = -rem * (b[1].m/b[0].m/3)**(1/3) # interior...
rfac = 1+dr0fid/rem
dx,dy,dz,dvx,dvy,dvz = drdv
b[tracerindex:].x,b[tracerindex:].y,b[tracerindex:].z = rfac*xem+xs+dx,rfac*yem+ys+dy,rfac*zem+zs+dz
vfac = 1+dr0fid/rem
b[tracerindex:].vx,b[tracerindex:].vy,b[tracerindex:].vz=vfac*vxem+vxs+dvx,vfac*vyem+vys+dvy,vfac*vzem+vzs+dvz
return
def norm2(x,y,z): return x**2+y**2+z**2
def skyang(b1,b2,bobs): # ang between b1 & b2 from b"obs"'s perspective
dx1,dy1.dz1=(b1.x-bobs.x),(b1.y-bobs.y),(b1.z-bobs.z)
dx2,dy2.dz2=(b2.x-bobs.x),(b2.y-bobs.y),(b2.z-bobs.z)
cosang = (dx1*dx2 + dy1*dy2 + dz1*dz2)/np.sqrt(norm2(dx1,dy1,dz1)*norm2(dx2,dy2,dz2))
return np.arccos(min(max(cosang,-1),1))
def unisphere(n,radius=1):
u = np.random.uniform(0,1,n) # uniform random vector of size nsamp
r = radius*np.cbrt(u)
phi = np.random.uniform(0,2*np.pi,n)
theta = np.arccos( np.random.uniform(-1,1,n) )
return r*np.sin(theta)*np.cos(phi),r*np.sin(theta)*np.sin(phi),r*np.cos(theta)
def powersphere(n,radius=1,gamma=1): # rho = r^-gamma
u = np.random.uniform(0,1,n) # uniform random vector of size nsamp
r = radius*u**(1/(3-gamma))
phi = np.random.uniform(0,2*np.pi,n)
theta = np.arccos( np.random.uniform(-1,1,n) )
return r*np.sin(theta)*np.cos(phi),r*np.sin(theta)*np.sin(phi),r*np.cos(theta)
# funcs to find L1....
def dist2lineEarthSun(b,tracerindex=-1):
xe,ye,ze = b[1].x-b[0].x,b[1].y-b[0].y,b[1].z-b[0].z # Earth rel Sun
xt,yt,zt = b[tracerindex:].x-b[0].x,b[tracerindex:].y-b[0].y,b[tracerindex:].z-b[0].z # tracer rel sun
q = (xt*xe+yt*ye+zt*ze)/(xe**2+ye**2+ze**2) # distance to the Earth-Sun line (not Earth+moon - Sun)
dist_to_line = np.sqrt((xe*q-xt)**2 + (ye*q-yt)**2 + (ze*q-zt)**2)
return dist_to_line
def dist2Earth(b,tracerindex=-1):
xt,yt,zt = b[tracerindex].x-b[1].x,b[tracerindex].y-b[1].y,b[tracerindex].z-b[1].z # tracer rel sun
dist_to_point = np.sqrt((xt)**2 + (yt)**2 + (zt)**2)
return dist_to_point
def halotrack(drdv,b0,tracerindex=-1,trun=1*yr,nt=3000):
b = b0.copy()
re = pairsep(b[1],b[0])
setorb(b,drdv,nb)
nsub = 200
percentrhill = re * (b[1].m/b[0].m/3)**(1/3) * 0.01
istarttrack = 0 # 0 to track very substep
tsub, ntsub = trun/nsub,nt//nsub
retval = 0.0
d2E,d2ES = [],[]
for i in range(nsub):
steps(b,tsub,ntsub)
if (i>=istarttrack):
d2E.append(dist2Earth(b,tracerindex))
d2ES.append(dist2lineEarthSun(b,tracerindex))
d2E,d2ES = np.array(d2E),np.array(d2ES)
retval = np.mean((d2ES/percentrhill)**4) # + np.std(d2E)**2
#retval = np.sqrt(np.mean((d2ES/percentrhill)**2)) # + np.std(d2E)**2
#print('xxx',b[1].x/AU,b[1].y/AU,b[1].vx,b[1].vy,'zzz',L1test(b,dr0))
print('xxx [%1.13e, %1.13e, %1.13e, %1.13e, %1.13e, %1.13e] %g '%(drdv[0],drdv[1],drdv[2],drdv[3],drdv[4],drdv[5],retval))
# print('xxx',b[tracerindex].x/AU,b[tracerindex].y/AU,b[tracerindex].vx,b[tracerindex].vy,'zzz %g'%retval)
return retval
def skycoords(b,tracerindex=3,loc='C'):
# this is overkill. create a basis, ux,uy,uz ux is earth-to-sun, uy is toward earth velocity, z is "up"
ex,ey,ez = b[1].x,b[1].y,b[1].z # earth pos (loc=='C' for center)
if loc in 'NSEW':
if loc == 'N': ez += b[1].r
elif loc == 'S': ez -= b[1].r
else:
sgn = 1 if loc=='W' else -1
evx,evy = b[1].vx,b[1].vy; fac = b[1].r/np.sqrt(evx**2+evy**2)
ex += sgn*evx*fac; ey += sgn*evy*fac;
dx,dy,dz = (b[tracerindex:].x-ex),(b[tracerindex:].y-ey),(b[tracerindex:].z-ez)
rp = np.sqrt(dx**2 + dy**2 + dz**2)
upx,upy,upz = dx/rp,dy/rp,dz/rp
dxs,dys,dzs = (b[0].x-ex),(b[0].y-ey),(b[0].z-ez) # sun pos in earth frame
re = np.sqrt(dxs**2+dys**2+dzs**2)
uxx,uxy,uxz = dxs/re,dys/re,dzs/re # unit vec, ux is x-like, dir of sun
uzx,uzy,uzz = (uxy*b[1].vz-uxz*b[1].vy),(uxz*b[1].vx-uxx*b[1].vz),(uxx*b[1].vy-uxy*b[1].vx)
unorm = np.sqrt(uzx**2+uzy**2+uzz**2); uzx,uzy,uzz = uzx/unorm,uzy/unorm,uzz/unorm # uz is z-like, perp to orb plane
uyx,uyy,uyz = (uzy*uxz-uzz*uxy),(uzz*uxx-uzx*uxz),(uzx*uxy-uzy*uxx)
unorm = np.sqrt(uyx**2+uyy**2+uyz**2); uyx,uyy,uyz = uyx/unorm,uyy/unorm,uyz/unorm # uy is y-like,
th = np.pi/2 - np.arccos(upx*uzx + upy*uzy + upz*uzz) # pi/2 - cosine angle, angle in z dir
ph = np.pi/2 - np.arccos(upx*uyx + upy*uyy + upz*uyz) #
# check if not near sun?
cossp = upx*uxx + upy*uxy + upz*uxz
th = np.where(cossp<0,np.pi-th,th)
ph = np.where(cossp<0,np.pi-ph,ph)
return th,ph
def earthsunframe(b,tracerindex=3):
# this is overkill. create a basis, ux,uy,uz ux is earth-to-sun, uy is toward earth velocity, z is "up"
ex,ey,ez = b[1].x,b[1].y,b[1].z # earth pos (loc=='C' for center)
dx,dy,dz = (b[tracerindex:].x-ex),(b[tracerindex:].y-ey),(b[tracerindex:].z-ez)
dxs,dys,dzs = (b[0].x-ex),(b[0].y-ey),(b[0].z-ez) # sun pos in earth frame
re = np.sqrt(dxs**2+dys**2+dzs**2); uxx,uxy,uxz = dxs/re,dys/re,dzs/re # ux, x-like, dir of sun
uzx,uzy,uzz = (uxy*b[1].vz-uxz*b[1].vy),(uxz*b[1].vx-uxx*b[1].vz),(uxx*b[1].vy-uxy*b[1].vx)
unorm = np.sqrt(uzx**2+uzy**2+uzz**2); uzx,uzy,uzz = uzx/unorm,uzy/unorm,uzz/unorm # uz, perp to orb plane
uyx,uyy,uyz = (uzy*uxz-uzz*uxy),(uzz*uxx-uzx*uxz),(uzx*uxy-uzy*uxx)
unorm = np.sqrt(uyx**2+uyy**2+uyz**2); uyx,uyy,uyz = uyx/unorm,uyy/unorm,uyz/unorm # uy is y-like
x,y,z = uxx*dx+uxy*dy+uxz*dz, uyx*dx+uyy*dy+uyz*dz, uzx*dx+uzy*dy+uzz*dz
return x,y,z
def cossep(bA,bB,b0):
xA,yA,zA = (bA.x-b0.x),(bA.y-b0.y),(bA.z-b0.z),
xB,yB,zB = (bB.x-b0.x),(bB.y-b0.y),(bB.z-b0.z),
cosp = (xA*xB+yA*yB+zA*zB)/np.sqrt((xA**2+yA**2+zA**2)*(xB**2+yB**2+zB**2))
return cosp
def overlap(rbig,rsmall,offset): #fraction of big circle that is partially overlapped by little circle
R,r,d = rbig,rsmall,offset # wolfram mathworld
drRfac,dRrfac = (d**2+r**2-R**2)/(2*d*r), (d**2+R**2-r**2)/(2*d*R)
drRfac = np.where(np.abs(drRfac)>1,drRfac/np.abs(drRfac),drRfac)
dRrfac = np.where(np.abs(dRrfac)>1,dRrfac/np.abs(dRrfac),dRrfac)
drRyuk = (-d+r+R)*(d+r-R)*(d-r+R)*(d+r+R)
drRyuk = np.where(drRyuk<0,0,drRyuk)
return (r**2*np.arccos(drRfac)+R**2*np.arccos(dRrfac)-0.5*np.sqrt(drRyuk))/(np.pi*R**2)
def radredux(b):
des,det,dst = pairsep(b[0],b[1]),pairsep(b,b[1]),pairsep(b,b[0])
f = np.zeros(len(b))
msk = (b.m<1e11)&(des>0)&(det>0)&(det<des) # should be all tracers
re,rs = b[1].r,b[0].r
rshadow = rs*det[msk]/(des-det[msk])
rshctr = des*np.sin(np.arccos(cossep(b[msk],b[1],b[0]))) # loc of tracer shadow in plane of earth disk
f[msk] = np.where((rshadow>re)&(rshctr<(rshadow-re)),re**2/rshadow**2,f[msk])
f[msk] = np.where((rshadow>re)&(rshctr>(rshadow-re)),overlap(rshadow,re,rshctr),f[msk])
f[msk] = np.where((rshadow<re)&(rshctr<(re-rshadow)),rshadow**2/re**2,f[msk])
f[msk] = np.where((rshadow<re)&(rshctr>(re-rshadow)),overlap(re,rshadow,rshctr),f[msk])
return f
def radreduxMC(b):
N = 5000; xg = np.linspace(-1,1,N)
dX,dY = np.meshgrid(xg,xg); msk = dX**2+dY**2 < 1; dX,dY = dX[msk].flatten(), dY[msk].flatten()
dA = 4/N**2+0*dX
re,rs = b[1].r,b[0].r
f = np.zeros(len(b))
for i in range(len(b)):
bi = b[i]
if (bi.m>1e11): continue
des,det,dst = pairsep(b[0],b[1]),pairsep(bi,b[1]),pairsep(bi,b[0])
rshadow = rs*det/(des-det)
rshctr = des*np.sin(np.arccos(cossep(bi,b[1],b[0])))
xi,yi,ai = dX*rshadow+rshctr,dY*rshadow,dA*rshadow**2
f[i] = (np.sum(ai[xi**2+yi**2<re**2])/(np.pi*rshadow**2))
return f
def ovrlap(d,re,rs): # overlapping area of circles rs > re displaced from centers by distance d.
return re**2*np.arccos((d**2+re**2-rs**2)/(2*d*re))+rs**2*np.arccos((d**2+rs**2-re**2)/(2*d*rs))\
-0.5*np.sqrt((d+re+rs)*(d-re+rs)*(d+re-rs)*(-d+re+rs))
def attengeo(rp,ang,d1=0.01*AU,asemi=AU):
global Rearth, Rsun
rs = Rsun*d1/(asemi-d1)
re = Rearth
d = ang*d1*asemi/(asemi-d1)
if np.isscalar(ang):
if d<=rs-re:
fs = re**2/rs**2
elif (d<rs+re)&(d>rs-re):
#print('xxx',d/re,rs/re)
fs = ovrlap(d,re,rs)/(np.pi*rs**2)
else:
fs = 0.0
else:
fs = np.where(d<=rs-re,re**2/rs**2,0)
msk = (d<rs+re)&(d>rs-re);
fs[msk] = ovrlap(d[msk],re,rs)/(np.pi*rs**2)
return fs*rp**2/d1**2*asemi**2/Rsun**2
def britensca(rp,th,g,nu,d1=0.01*AU,asemi=AU):
global Rearth, Rsun
delOm = np.pi*(Rearth/d1)**2
return rp**2/d1**2*sc.phase_function_D03(th,g,nu)*delOm*asemi**2/Rsun**2
def puff(bref,ntracer, R = 1*km, puffspeed = 0, puffdisp = 60, ang = 30*np.pi/180., rp = 1e-4, rhop = 2.7):
mp = 4*np.pi*rhop*rp**3
bt = np.array([bref]*(ntracer),dtype=b.dtype).view(np.recarray)
dr = np.array(unisphere(ntracer,radius=R)) if R>0 else 0
bt.x, bt.y, bt.z = np.array([bt.x,bt.y,bt.z]) + dr
erad = np.array([bref.x,bref.y,bref.z]*ntracer).reshape((ntracer,3)).T/dist(bref)
#print(erad.shape)
evel = np.array([bref.vx,bref.vy,bref.vz]*ntracer).reshape((ntracer,3)).T/speed(bref)
ezed = np.array([0,0,1]*ntracer).T
dv = puffspeed * (np.cos(ang)*evel - np.sin(ang)*erad) + np.random.normal(0,puffdisp,(3,ntracer))
dv[2,:] *= 1
bt.vx, bt.vy, bt.vz = np.array([bt.vx,bt.vy,bt.vz]) + dv
bt.r,bt.m = rp,mp
return bt
def mycloud(bref,ntracer,rS = 100e2, vs = 0, rp = 1e-4, rhop = 2.7):
mp = 4*np.pi*rhop*rp**3
bt = np.array([bref]*(ntracer),dtype=b.dtype).view(np.recarray)
dr = np.array(unisphere(ntracer,radius=rS))
bt.x, bt.y, bt.z = np.array([bt.x,bt.y,bt.z]) + dr
dv = dr*vs/rS
bt.vx, bt.vy, bt.vz = np.array([bt.vx,bt.vy,bt.vz]) + dv
bt.r,bt.m = rp,mp
return bt
def dumpmxv(nm,b):
for nmi,bi in zip(nm,b):
print('%s & %13.10e & %13.10f & %13.10f & %13.10f & %13.10f & %13.10f & %13.10f \\\\' % \
(nmi,bi.m/1e3,bi.x/AU,bi.y/AU,bi.z/AU,bi.vx/km,bi.vy/km,bi.vz/km))
# ---- Main -----
np.random.seed(94123421)
fil = 'solarsystem.csv'
dfsolsys = pd.read_csv(fil)
sun = dfsolsys.iloc[0]
earth = dfsolsys.iloc[3]
moon = dfsolsys.iloc[4]
venus = dfsolsys.iloc[2]
mars = dfsolsys.iloc[5]
jupiter = dfsolsys.iloc[6]
saturn = dfsolsys.iloc[7]
nm = ['Sun','Earth','Moon','Venus','Mars','Jupiter','Saturn']
nb = 3 # number of massive nbodies
nb = 7 # include nearby, big planets
b = np.zeros(nb+1,dtype=bodyt).view(np.recarray)
b[0] = (sun.m,sun.r,sun.x,sun.y,sun.z,sun.vx,sun.vy,sun.vz,0,0,0,0,0)
b[1] = (earth.m,earth.r,earth.x,earth.y,earth.z,earth.vx,earth.vy,earth.vz,0,0,0,0,0)
b[2] = (moon.m,moon.r,moon.x,moon.y,moon.z,moon.vx,moon.vy,moon.vz,0,0,0,0,0)
if nb>3: b[3] = (venus.m,venus.r,venus.x,venus.y,venus.z,venus.vx,venus.vy,venus.vz,0,0,0,0,0)
if nb>4: b[4] = (mars.m,mars.r,mars.x,mars.y,mars.z,mars.vx,mars.vy,mars.vz,0,0,0,0,0)
if nb>5: b[5] = (jupiter.m,jupiter.r,jupiter.x,jupiter.y,jupiter.z,jupiter.vx,jupiter.vy,jupiter.vz,0,0,0,0,0)
if nb>6: b[6] = (saturn.m,saturn.r,saturn.x,saturn.y,saturn.z,saturn.vx,saturn.vy,saturn.vz,0,0,0,0,0)
ti = tracerindex = nb
bm = b[:nb] # all massive....
comr = np.sum(np.array([bm.m*bm.x,bm.m*bm.y,bm.m*bm.z])/np.sum(bm.m),axis=1)
comv = np.sum(np.array([bm.m*bm.vx,bm.m*bm.vy,bm.m*bm.vz])/np.sum(bm.m),axis=1)
b.x -= comr[0]; b.y -= comr[1]; b.z -= comr[2];
b.vx -= comv[0]; b.vy -= comv[1]; b.vz -= comv[2];
dr0fid = -pairsep(b[1],b[0])*(b.m[1]/3/b.m[0])**(1./3)
dr0 = dr0fid
# for solar eclipse of 2017
drdv = np.array([9.87060899e+07, 9.94944750e+07, 1.01205252e+06, 1.01626852e+01,
1.01174070e+01, 9.99609883e+01]) # cute solution optimized on square of dist to Earth-Sun Line....
drdv = np.array([9.7819160134069e+07, 1.0086054786768e+08, 1.0406685899666e+06, 1.0386484846233e+01, 9.8161719507052e+00, 9.7691723511862e+01]) # best quad, still "cute"...grr i thought i had a better one...
drdv = np.array([9.7672356395251e+07, 1.0145546625866e+08, 1.0474139184824e+05, 1.0271868687687e+01, 9.7177468883876e+00, 9.7381395186548e+00]) # best quad
setorb(b,drdv,tracerindex=ti)
bstart = b.copy()
do_fit = False
# do_fit = True
if do_fit:
tfit = 1.0*yr
mytol = 4e-3
mytol = 0.004
mytest = halotrack(drdv,b,ti,tfit,4000)
print('# my test:',mytest)
print('# L1 dist: ',pairsep(b[-1],b[1])/pairsep(b[-1],b[0]))
if mytest > mytol:
smplx = [drdv]
for j in range(1,7):
u = np.random.uniform(0.9,1.1,len(drdv))
u = np.random.uniform(0.99,1.01,len(drdv))
smplx.append(u*drdv)
smplx = np.array(smplx)
maxiter = 400
res = minimize(halotrack,drdv,args=(b,ti,1.0*tfit,4000),method='Nelder-Mead',
options={'maxiter':maxiter, 'fatol':0.1,'initial_simplex':smplx})
print(res)
drdv = res.x
setorb(b,drdv,nb)
bstart = b.copy()
else:
print('L1 test metric',mytest)
print('# sun-tracer dist/AU:',pairsep(b[ti],b[0])/AU)
print('# earth-tracer dist/AU:',pairsep(b[ti],b[1])/AU)
print('# moon-tracer dist/AU:',pairsep(b[ti],b[2])/AU)
print('# earth-sun dist/AU:',pairsep(b[0],b[1])/AU)
print('# moon-sun dist/AU:',pairsep(b[0],b[2])/AU)
ntracer = 1000
gdraine,nudraine = 0.0,0.5
hh = np.linspace(0,np.pi,10000); ddhh = hh[1]-hh[0]
gg = np.sum(sc.phase_function_F19(hh)*np.sin(hh)*np.cos(hh)*2*np.pi*ddhh)
#Rshadow = b[0].r*np.abs(dr0fid)/(pairsep(b[0],b[1])-np.abs(dr0fid))
#print(Rshadow,Rshadow/b[1].r)
make_movie = False
plot_traj = False
do_it = False
plot_beta = False
mode = 'traj'
#mode = 'beta'
#mode = 'movie'
if 'movie' in mode:
make_movie = True
if 'traj' in mode:
plot_traj = True
if 'beta' in mode:
plot_beta = True
if 'do_it' in mode:
do_it = True
# defaults for plot_traj
ntracer = 1
tmax = 1.0*yr
#ddt = 1*yr/16000
ddt = 1*yr/8000
npl = 400 # numper of plot calls
rhop = 2.7
rp = 1e-4
if make_movie:
rp = 1e3*1e-1
ntracer = 20000
create_cloud = True
if plot_beta:
print('overiding parms to plot orbits for different beta...')
ntracer = 6
tmax = 28*24*3600
b = np.append(b,mycloud(b[ti],ntracer-1)).view(np.recarray)
b[ti+1:].r = np.logspace(-3,-1,ntracer-1)
b[ti+1:].r = np.array([10e-4,32e-4,100e-4,320e-4,0.1])
b[ti+1:].m = 4*np.pi/3*rhop*b[ti+1:].r**3
b[ti+1:].Q = 1-gdraine
b[ti+1:].eta = 1/3.
tracerdat = np.zeros((npl,ntracer*3))
if do_it:
print('overiding parms to do do_it...')
ntracer = 10
tmax = 0.1*yr
b = np.append(b,mycloud(b[ti],ntracer-1)).view(np.recarray)
b[ti+1:].r = np.logspace(-4,0,ntracer-1)
b[ti+1:].Q = 1
b[ti+1:].eta = 1/3.
bstart = b.copy()
Estart = energy(bstart)
dt = tmax/npl
ntsub = int(dt/ddt)+1
tstart = time.time()
phlis = np.zeros(3)
L = 1.0*np.pi/180
na = 600
ell = np.linspace(-0.5*L,0.5*L,na)
dell = ell[1]-ell[0]
elledge = np.linspace(-0.5*(L+dell),0.5*(L+dell),na+1)
X,Y = np.meshgrid(ell,ell)
if make_movie:
cmap = 'gnuplot2'
csky,csun = -0.75,0.96 # color vals working off of whatever cmap
csky,csun = 0.5,0.96 # color vals working off of whatever cmap
cmap = 'gist_gray'
fmovcstr = 'tmp'+str(os.getpid())+'*.png'
# print(glob.glob(fmovcstr))
if len(glob.glob(fmovcstr))>0:
print('# removing files',fmovcstr)
os.system('rm '+fmovcstr)
thph = []
thphN,thphS,thphE,thphW = [],[],[],[]
attnlis = []
radpress = True
nm = nm + ['tracer']*(len(b)-7)
dumpmxv(nm,b)
for i in range(npl):
steps(b,dt,ntsub)
print(energy(b),energy(bstart))
re = pairsep(b[1],b[0])
tnow = dt*(i+1)
if make_movie:
thti,phti = skycoords(b[:ti+1],ti)
if create_cloud:
bp = puff(b[ti],ntracer//npl, R=0, puffdisp=30, rp=b[ti].r,rhop=rhop)
bp.r += np.random.normal(0,0.01*b[ti].r,ntracer//npl)
b = np.append(b,bp).view(np.recarray)
Z = 0*X + csky
msk = X**2 + Y**2 < (Rsun/re)**2; Z[msk] = csun
th,ph = skycoords(b,ti)
ZZ,_,_ = np.histogram2d(th,ph,bins=[elledge,elledge],)
Z = np.where(ZZ>0,-1,Z)
pl.imshow(Z,extent=(elledge[0],elledge[-1],elledge[0],elledge[-1]),cmap=cmap,vmin=-1,vmax=1)
#pl.scatter(phti*180/np.pi,thti*180/np.pi,c='#ffffff',s=10)
pl.figtext(0.6,0.2,'%0.3f'%(tnow/yr),color='#660066')
out = fmovcstr.replace('*','%04d')%(i)
print('# saving',out)
noccult = np.sum(ZZ[msk])
print('# this time, n tot, n occult:',tnow/yr,len(b),noccult)
pl.savefig(out)
pl.clf()
if plot_beta:
xt,yt,zt = earthsunframe(b,ti)
tracerdat[i] = np.concatenate((xt,yt,zt))
print(tnow/yr,'beta...')
if plot_traj:
th, ph = skycoords(b[:ti+1],ti)
nC = np.sum(np.sqrt(th**2+ph**2)<b[0].r/pairsep(b[1],b[0]))
#neffMC = np.sum(radreduxMC(b[:ti+1]))
#neff = np.sum(radredux(b))
thph.append([tnow,th[0],ph[0]])
print(tnow/yr,nC)
if do_it:
#print(b[ti:])
lat, lon = skycoords(b,tracerindex=ti)
ang = np.sqrt(lat**2+lon**2)[0]
attn = attengeo(1.0,ang,d1=0.01*AU,asemi=AU)
bri = britensca(1.0,ang,gdraine,nudraine,d1=0.01*AU,asemi=AU)
attnlis.append(np.sum(attn-bri))
afac = (1/Rsun**2*AU**2/(0.01*AU)**2)
print('# attn,bri,net of L1 tracer:',attn/afac,bri/afac,(attn-bri)/afac)
ZZ,_,_ = np.histogram2d(lat,lon,bins=[elledge,elledge],)
nzz = np.sum(ZZ)
print('zz stats',np.min(ZZ),np.mean(ZZ),np.max(ZZ),np.sum(ZZ))
print("# looptime %s s"%(time.time()-tstart))
Estart = energy(bstart)
Efinal = energy(b)
print('frac energy error:',np.abs((Efinal-Estart)/Estart))
if do_it:
attnlis = np.array(attnlis)
afac = (1/Rsun**2*AU**2/(0.01*AU)**2)
attnmean,attnmin,attnmax = np.mean(attnlis),np.min(attnlis),np.max(attnlis)
attnmean /= afac; attnmin /= afac; attnmax /= afac;
print("# attenuation summary: mean min max:",attnmean,attnmin,attnmax)
if make_movie:
os.system('convert '+fmovcstr+' ~/public_html/tmp.gif')
print('# removing files',fmovcstr)
os.system('rm '+fmovcstr)
if plot_beta:
#pl.gca().set_aspect('equal')
#aa = np.linspace(0,2*np.pi,100)
#xx,yy = b[1].r * np.cos(aa) ,b[1].r*np.sin(aa)
#pl.plot(xx,yy,'-',c='#999999')
#pl.scatter([0],[0],s=5,c='#999999')
xmax = 0
for i in range(1,ntracer):
xt,yt = (tracerdat[:,i]-tracerdat[:,0])/Rearth,(tracerdat[:,ntracer+i]-tracerdat[:,ntracer])/Rearth
xt *= -1
rt = b[ti+i].r
if 1:
if rt >= 0.1:
label = '%1.0f mm'%(rt/1e-1)
else:
label = '%1.0f $\mu$m'%(rt/1e-4)
pl.plot(xt,yt,'-', c='k',alpha=i/(ntracer-1),label=label)
else:
pl.plot(xt,yt,'-', c='k',alpha=i/(ntracer-1))
xmax = np.max(xt)
pl.xlim(-1,20)
pl.ylim(-4.5,1.5)
pl.xlabel(r'x (R$_\oplus$)',size=14)
pl.ylabel(r'y (R$_\oplus$)',size=14)
pl.legend()
out = 'halojplbeta.pdf'
pl.savefig(out)
os.system('convert '+out+' ~/public_html/tmp.jpg')
if plot_traj:
dumpmxv(nm,b)
re = pairsep(b[1],b[0])
angsun = (b[0].r/re)*180/np.pi
aa = np.linspace(0,2*np.pi,100)
xx,yy = angsun*np.cos(aa),angsun*np.sin(aa)
pl.gca().set_aspect('equal')
pl.plot(xx,yy,'-',c='#999999')
pl.xlabel(r'$\Delta\phi$ (deg)',size=14)
pl.ylabel(r'$\Delta\theta$ (deg)',size=14)
out = 'halojpltraj.pdf'
print('dumping to',out)
ts,th,ph = np.array(thph).T
hint,pint = interp1d(ts,th),interp1d(ts,ph)
tsi = np.linspace(ts[0],ts[-1],len(ts)*10)
thi, phi = hint(tsi), pint(tsi)
pl.scatter(phi*180/np.pi,thi*180/np.pi,s=0.25,c=tsi,cmap='binary')
pl.savefig(out)
os.system('convert '+out+' ~/public_html/tmp.jpg')
myscript = __file__
fignm = myscript.split('_')[1]
print(fignm)
pl.savefig(fignm+".pdf")
pclm_Fig3_persistjpl.py 0000644 0501442 0003262 00000032216 14326612071 014774 0 ustar u0095165 bromley #
import numpy as np
import pandas as pd
from scipy.optimize import minimize
from scipy.interpolate import interp1d
import time
import pylab as pl
import os
import glob
from nbody import *
import myfig
from constants import *
G = GNewt
def setorb(b,drdv,tracerindex=3): # reconsider returning, not this crap
xs,ys,zs = b[0].x,b[0].y,b[0].z
vxs,vys,vzs = b[0].vx,b[0].vy,b[0].vz
# work in sun frame
xem = np.sum((b[1:3].x-xs)*b[1:3].m)/np.sum(b[1:3].m)
yem = np.sum((b[1:3].y-ys)*b[1:3].m)/np.sum(b[1:3].m)
zem = np.sum((b[1:3].z-zs)*b[1:3].m)/np.sum(b[1:3].m)
rem = np.sqrt(xem**2+yem**2+zem**2)
vxem = np.sum((b[1:3].vx-vxs)*b[1:3].m)/np.sum(b[1:3].m)
vyem = np.sum((b[1:3].vy-vys)*b[1:3].m)/np.sum(b[1:3].m)
vzem = np.sum((b[1:3].vz-vzs)*b[1:3].m)/np.sum(b[1:3].m)
#dr0 = -rem*(b[1].m/3/b[0].m)**(1/3)
dr0fid = -rem * (b[1].m/b[0].m/3)**(1/3) # interior...
rfac = 1+dr0fid/rem
dx,dy,dz,dvx,dvy,dvz = drdv
b[tracerindex:].x,b[tracerindex:].y,b[tracerindex:].z = rfac*xem+xs+dx,rfac*yem+ys+dy,rfac*zem+zs+dz
vfac = 1+dr0fid/rem
b[tracerindex:].vx,b[tracerindex:].vy,b[tracerindex:].vz=vfac*vxem+vxs+dvx,vfac*vyem+vys+dvy,vfac*vzem+vzs+dvz
return
def norm2(x,y,z): return x**2+y**2+z**2
def skyang(b1,b2,bobs): # ang between b1 & b2 from b"obs"'s perspective
dx1,dy1.dz1=(b1.x-bobs.x),(b1.y-bobs.y),(b1.z-bobs.z)
dx2,dy2.dz2=(b2.x-bobs.x),(b2.y-bobs.y),(b2.z-bobs.z)
cosang = (dx1*dx2 + dy1*dy2 + dz1*dz2)/np.sqrt(norm2(dx1,dy1,dz1)*norm2(dx2,dy2,dz2))
return np.arccos(min(max(cosang,-1),1))
def unisphere(n,radius=1):
u = np.random.uniform(0,1,n) # uniform random vector of size nsamp
r = radius*np.cbrt(u)
phi = np.random.uniform(0,2*np.pi,n)
theta = np.arccos( np.random.uniform(-1,1,n) )
return r*np.sin(theta)*np.cos(phi),r*np.sin(theta)*np.sin(phi),r*np.cos(theta)
def powersphere(n,radius=1,gamma=1): # rho = r^-gamma
u = np.random.uniform(0,1,n) # uniform random vector of size nsamp
r = radius*u**(1/(3-gamma))
phi = np.random.uniform(0,2*np.pi,n)
theta = np.arccos( np.random.uniform(-1,1,n) )
return r*np.sin(theta)*np.cos(phi),r*np.sin(theta)*np.sin(phi),r*np.cos(theta)
# funcs to find L1....
def dist2lineEarthSun(b,tracerindex=-1):
xe,ye,ze = b[1].x-b[0].x,b[1].y-b[0].y,b[1].z-b[0].z # Earth rel Sun
xt,yt,zt = b[tracerindex:].x-b[0].x,b[tracerindex:].y-b[0].y,b[tracerindex:].z-b[0].z # tracer rel sun
q = (xt*xe+yt*ye+zt*ze)/(xe**2+ye**2+ze**2) # distance to the Earth-Sun line (not Earth+moon - Sun)
dist_to_line = np.sqrt((xe*q-xt)**2 + (ye*q-yt)**2 + (ze*q-zt)**2)
return dist_to_line
def dist2Earth(b,tracerindex=-1):
xt,yt,zt = b[tracerindex].x-b[1].x,b[tracerindex].y-b[1].y,b[tracerindex].z-b[1].z # tracer rel sun
dist_to_point = np.sqrt((xt)**2 + (yt)**2 + (zt)**2)
return dist_to_point
def skycoords(b,tracerindex=3,loc='C'):
# this is overkill. create a basis, ux,uy,uz ux is earth-to-sun, uy is toward earth velocity, z is "up"
ex,ey,ez = b[1].x,b[1].y,b[1].z # earth pos (loc=='C' for center)
if loc in 'NSEW':
if loc == 'N': ez += b[1].r
elif loc == 'S': ez -= b[1].r
else:
sgn = 1 if loc=='W' else -1
evx,evy = b[1].vx,b[1].vy; fac = b[1].r/np.sqrt(evx**2+evy**2)
ex += sgn*evx*fac; ey += sgn*evy*fac;
dx,dy,dz = (b[tracerindex:].x-ex),(b[tracerindex:].y-ey),(b[tracerindex:].z-ez)
rp = np.sqrt(dx**2 + dy**2 + dz**2)
upx,upy,upz = dx/rp,dy/rp,dz/rp
dxs,dys,dzs = (b[0].x-ex),(b[0].y-ey),(b[0].z-ez) # sun pos in earth frame
re = np.sqrt(dxs**2+dys**2+dzs**2)
uxx,uxy,uxz = dxs/re,dys/re,dzs/re # unit vec, ux is x-like, dir of sun
uzx,uzy,uzz = (uxy*b[1].vz-uxz*b[1].vy),(uxz*b[1].vx-uxx*b[1].vz),(uxx*b[1].vy-uxy*b[1].vx)
unorm = np.sqrt(uzx**2+uzy**2+uzz**2); uzx,uzy,uzz = uzx/unorm,uzy/unorm,uzz/unorm # uz is z-like, perp to orb plane
uyx,uyy,uyz = (uzy*uxz-uzz*uxy),(uzz*uxx-uzx*uxz),(uzx*uxy-uzy*uxx)
unorm = np.sqrt(uyx**2+uyy**2+uyz**2); uyx,uyy,uyz = uyx/unorm,uyy/unorm,uyz/unorm # uy is y-like,
th = np.pi/2 - np.arccos(upx*uzx + upy*uzy + upz*uzz) # pi/2 - cosine angle, angle in z dir
ph = np.pi/2 - np.arccos(upx*uyx + upy*uyy + upz*uyz) #
# check if not near sun?
cossp = upx*uxx + upy*uxy + upz*uxz
th = np.where(cossp<0,np.pi-th,th)
ph = np.where(cossp<0,np.pi-ph,ph)
return th,ph
def earthsunframe(b,tracerindex=3):
# this is overkill. create a basis, ux,uy,uz ux is earth-to-sun, uy is toward earth velocity, z is "up"
ex,ey,ez = b[1].x,b[1].y,b[1].z # earth pos (loc=='C' for center)
dx,dy,dz = (b[tracerindex:].x-ex),(b[tracerindex:].y-ey),(b[tracerindex:].z-ez)
dxs,dys,dzs = (b[0].x-ex),(b[0].y-ey),(b[0].z-ez) # sun pos in earth frame
re = np.sqrt(dxs**2+dys**2+dzs**2); uxx,uxy,uxz = dxs/re,dys/re,dzs/re # ux, x-like, dir of sun
uzx,uzy,uzz = (uxy*b[1].vz-uxz*b[1].vy),(uxz*b[1].vx-uxx*b[1].vz),(uxx*b[1].vy-uxy*b[1].vx)
unorm = np.sqrt(uzx**2+uzy**2+uzz**2); uzx,uzy,uzz = uzx/unorm,uzy/unorm,uzz/unorm # uz, perp to orb plane
uyx,uyy,uyz = (uzy*uxz-uzz*uxy),(uzz*uxx-uzx*uxz),(uzx*uxy-uzy*uxx)
unorm = np.sqrt(uyx**2+uyy**2+uyz**2); uyx,uyy,uyz = uyx/unorm,uyy/unorm,uyz/unorm # uy is y-like
x,y,z = uxx*dx+uxy*dy+uxz*dz, uyx*dx+uyy*dy+uyz*dz, uzx*dx+uzy*dy+uzz*dz
return x,y,z
def cossep(bA,bB,b0):
xA,yA,zA = (bA.x-b0.x),(bA.y-b0.y),(bA.z-b0.z),
xB,yB,zB = (bB.x-b0.x),(bB.y-b0.y),(bB.z-b0.z),
cosp = (xA*xB+yA*yB+zA*zB)/np.sqrt((xA**2+yA**2+zA**2)*(xB**2+yB**2+zB**2))
return cosp
def overlap(rbig,rsmall,offset): #fraction of big circle that is partially overlapped by little circle
R,r,d = rbig,rsmall,offset # wolfram mathworld
drRfac,dRrfac = (d**2+r**2-R**2)/(2*d*r), (d**2+R**2-r**2)/(2*d*R)
drRfac = np.where(np.abs(drRfac)>1,drRfac/np.abs(drRfac),drRfac)
dRrfac = np.where(np.abs(dRrfac)>1,dRrfac/np.abs(dRrfac),dRrfac)
drRyuk = (-d+r+R)*(d+r-R)*(d-r+R)*(d+r+R)
drRyuk = np.where(drRyuk<0,0,drRyuk)
return (r**2*np.arccos(drRfac)+R**2*np.arccos(dRrfac)-0.5*np.sqrt(drRyuk))/(np.pi*R**2)
def radredux(b):
des,det,dst = pairsep(b[0],b[1]),pairsep(b,b[1]),pairsep(b,b[0])
f = np.zeros(len(b))
msk = (b.m<1e11)&(des>0)&(det>0)&(det<des) # should be all tracers
re,rs = b[1].r,b[0].r
rshadow = rs*det[msk]/(des-det[msk])
rshctr = des*np.sin(np.arccos(cossep(b[msk],b[1],b[0]))) # loc of tracer shadow in plane of earth disk
f[msk] = np.where((rshadow>re)&(rshctr<(rshadow-re)),re**2/rshadow**2,f[msk])
f[msk] = np.where((rshadow>re)&(rshctr>(rshadow-re)),overlap(rshadow,re,rshctr),f[msk])
f[msk] = np.where((rshadow<re)&(rshctr<(re-rshadow)),rshadow**2/re**2,f[msk])
f[msk] = np.where((rshadow<re)&(rshctr>(re-rshadow)),overlap(re,rshadow,rshctr),f[msk])
return f
def radreduxMC(b):
N = 5000; xg = np.linspace(-1,1,N)
dX,dY = np.meshgrid(xg,xg); msk = dX**2+dY**2 < 1; dX,dY = dX[msk].flatten(), dY[msk].flatten()
dA = 4/N**2+0*dX
re,rs = b[1].r,b[0].r
f = np.zeros(len(b))
for i in range(len(b)):
bi = b[i]
if (bi.m>1e11): continue
des,det,dst = pairsep(b[0],b[1]),pairsep(bi,b[1]),pairsep(bi,b[0])
rshadow = rs*det/(des-det)
rshctr = des*np.sin(np.arccos(cossep(bi,b[1],b[0])))
xi,yi,ai = dX*rshadow+rshctr,dY*rshadow,dA*rshadow**2
f[i] = (np.sum(ai[xi**2+yi**2<re**2])/(np.pi*rshadow**2))
return f
def ovrlap(d,re,rs): # overlapping area of circles rs > re displaced from centers by distance d.
return re**2*np.arccos((d**2+re**2-rs**2)/(2*d*re))+rs**2*np.arccos((d**2+rs**2-re**2)/(2*d*rs))\
-0.5*np.sqrt((d+re+rs)*(d-re+rs)*(d+re-rs)*(-d+re+rs))
def attengeo(rp,ang,d1=0.01*AU,asemi=AU):
global Rearth, Rsun
rs = Rsun*d1/(asemi-d1)
re = Rearth
d = ang*d1*asemi/(asemi-d1)
if np.isscalar(ang):
if d<=rs-re:
fs = re**2/rs**2
elif (d<rs+re)&(d>rs-re):
#print('xxx',d/re,rs/re)
fs = ovrlap(d,re,rs)/(np.pi*rs**2)
else:
fs = 0.0
else:
fs = np.where(d<=rs-re,re**2/rs**2,0)
msk = (d<rs+re)&(d>rs-re);
fs[msk] = ovrlap(d[msk],re,rs)/(np.pi*rs**2)
return fs*rp**2/d1**2*asemi**2/Rsun**2
def puff(bref,ntracer, R = 1*km, puffspeed = 0, puffdisp = 60, ang = 30*np.pi/180., rp = 1e-4, rhop = 2.7):
mp = 4*np.pi*rhop*rp**3
bt = np.array([bref]*(ntracer),dtype=b.dtype).view(np.recarray)
dr = np.array(unisphere(ntracer,radius=R)) if R>0 else 0
bt.x, bt.y, bt.z = np.array([bt.x,bt.y,bt.z]) + dr
erad = np.array([bref.x,bref.y,bref.z]*ntracer).reshape((ntracer,3)).T/dist(bref)
#print(erad.shape)
evel = np.array([bref.vx,bref.vy,bref.vz]*ntracer).reshape((ntracer,3)).T/speed(bref)
ezed = np.array([0,0,1]*ntracer).T
dv = puffspeed * (np.cos(ang)*evel - np.sin(ang)*erad) + np.random.normal(0,puffdisp,(3,ntracer))
dv[2,:] *= 1
bt.vx, bt.vy, bt.vz = np.array([bt.vx,bt.vy,bt.vz]) + dv
bt.r,bt.m = rp,mp
return bt
def mycloud(bref,ntracer,rS = 100e2, vs = 0, rp = 1e-4, rhop = 2.7):
mp = 4*np.pi*rhop*rp**3
bt = np.array([bref]*(ntracer),dtype=b.dtype).view(np.recarray)
dr = np.array(unisphere(ntracer,radius=rS))
bt.x, bt.y, bt.z = np.array([bt.x,bt.y,bt.z]) + dr
dv = dr*vs/rS
bt.vx, bt.vy, bt.vz = np.array([bt.vx,bt.vy,bt.vz]) + dv
bt.r,bt.m = rp,mp
return bt
# ---- Main -----
np.random.seed(94123421)
fil = 'solarsystem.csv'
dfsolsys = pd.read_csv(fil)
sun = dfsolsys.iloc[0]
earth = dfsolsys.iloc[3]
moon = dfsolsys.iloc[4]
venus = dfsolsys.iloc[2]
mars = dfsolsys.iloc[5]
jupiter = dfsolsys.iloc[6]
saturn = dfsolsys.iloc[7]
nb = 3 # number of massive nbodies
nb = 7 # include nearby, big planets
b = np.zeros(nb+1,dtype=bodyt).view(np.recarray)
b[0] = (sun.m,sun.r,sun.x,sun.y,sun.z,sun.vx,sun.vy,sun.vz,0,0,0,0,0)
b[1] = (earth.m,earth.r,earth.x,earth.y,earth.z,earth.vx,earth.vy,earth.vz,0,0,0,0,0)
b[2] = (moon.m,moon.r,moon.x,moon.y,moon.z,moon.vx,moon.vy,moon.vz,0,0,0,0,0)
if nb>3: b[3] = (venus.m,venus.r,venus.x,venus.y,venus.z,venus.vx,venus.vy,venus.vz,0,0,0,0,0)
if nb>4: b[4] = (mars.m,mars.r,mars.x,mars.y,mars.z,mars.vx,mars.vy,mars.vz,0,0,0,0,0)
if nb>5: b[5] = (jupiter.m,jupiter.r,jupiter.x,jupiter.y,jupiter.z,jupiter.vx,jupiter.vy,jupiter.vz,0,0,0,0,0)
if nb>6: b[6] = (saturn.m,saturn.r,saturn.x,saturn.y,saturn.z,saturn.vx,saturn.vy,saturn.vz,0,0,0,0,0)
ti = tracerindex = nb
bm = b[:nb] # all massive....
comr = np.sum(np.array([bm.m*bm.x,bm.m*bm.y,bm.m*bm.z])/np.sum(bm.m),axis=1)
comv = np.sum(np.array([bm.m*bm.vx,bm.m*bm.vy,bm.m*bm.vz])/np.sum(bm.m),axis=1)
b.x -= comr[0]; b.y -= comr[1]; b.z -= comr[2];
b.vx -= comv[0]; b.vy -= comv[1]; b.vz -= comv[2];
drdv = np.array([9.7672356395251e+07, 1.0145546625866e+08, 1.0474139184824e+05, 1.0271868687687e+01, 9.7177468883876e+00, 9.7381395186548e+00]) # best quad